Астрофизический семинар ИНАСАН № 84 (30 ноября 2004 г., 14:30)

Опубликовано: 30/11/2004

Докладчик: Xiangqun Cui (National Astronomical Observatories, China)

Название доклада: “LAMOST: The Large Sky Area Multi-Object Fiber Spectroscopic Telescope”

Краткое содержание доклада:
LAMOST is a meridian reflecting Schmidt telescope laid down on the ground with its optical axis fixed in the meridian plane. Both the primary mirror and the focal plane are fixed on their ground bases, and the reflecting corrector, as a coelostat, tracks the motion of celestial objects. The light of individual objects is fed into the front ends of optical fibers accurately positioned on the focal plane, and then transferred into the spectrographs fixed in the room underneath, to be dispersed into spectra and recorded on the CCD detectors, respectively and simultaneously. The primary mirror has a size of 6.67m x 6.05m with a radius of curvature of 40m, which consists of 37 hexagonal spherical submirrors, each of them having a diagonal of 1.1m and a thickness of 75mm. The reflecting corrector is located at the center of curvature of the primary mirror, and its size is 5.72m x 4.40m, which consists of 24 hexagonal plane submirrors, each of them having a diagonal of 1.1m and a thickness of 25mm. The clear aperture of the telescope is around 4m that would become a little larger or smaller depending on the declination of the sky to be observed. The system gives excellent image quality within the 5o field of view. The large focal plane of 1.75m in diameter, corresponding to the 5o field of view, may easily accommodate up to 4000 optical fibers. The spectroscopic survey carried out by LAMOST of tens of millions of galaxies and others will make substantial contribution to the study of extra-galactic astrophysics and cosmology, such as galaxies, quasars and the large-scale structure of the universe. Its spectroscopic survey of large number of stars will make substantial contribution to the study of stellar astrophysics and the Galaxy. The telescope will be located at the Xinglong station of Beijing Astronomical Observatory, CAS.